adsabs/AstroCLIMB huggingface dataset:
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Comparisons of the constraints to the ΛCDM (upper) and flat w 0 w  a CDM (lower) models assuming a logarithmic evolution (﹩\delta \mu =\hat{k}\mathrm{ln}(1+z)﹩) of the distance modulus with redshift. The contours are 1σ, 2σ and 3σ levels for the Pantheon with Planck prior (gray lines), Pantheon plus VHZ SNe and Planck prior (green lines), Pantheon with statistical errors reduced by a factor of 4 and a Planck prior (blue lines), and Pantheon with statistical errors reduced by a factor of 4 plus VHZ SNe (orange lines). The solid straight line on the upper panel shows the line for a flat universe. The solid dashed horizontal and vertical lines on the lower panel show the assumed values of the w 0 and w  a  for the simulated VHZ SN data.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: The upper and lower two panels show the model fits, assuming a linear and a logarithmic systematic evolution of the SN Ia distances, respectively. The left and right panels are for the ΛCDM and flat w 0 w  a CDM models, respectively. The contours are calculated for the combined binned Pantheon data and the VHZ SNe Ia. The titles of the corner plot boxes show the 1σ range of the parameters. The contour levels are 1σ, 2σ, and 3σ with decreasing color weight.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Same as Figures 3 and 6, but the statistical errors of the lower redshift SN sample are decreased artificially by a factor of 4.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Same as Figure 3, but the statistical errors of the lower redshift SN sample are reduced artificially by a factor of ﹩\sqrt{8}﹩.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Same as Figure 9, but combined with the Planck 2018 results.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: Same as in Figure 11 but combined with the Planck 2018 results.
Paper: The Small Separation A-star Companion Population: First Results with CHARA/MIRC-X
Authors: Matthew De Furio, Tyler Gardner, John Monnier, Michael R. Meyer, Kaitlin Kratter, Gail Schaefer, Narsireddy Anugu, Claire L. Davies, Stefan Kraus, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Jacob Ennis
Figure caption: Companion frequencies based on spectral type of the primary star from the various models listed in Section 4.2. All frequencies are calculated over mass ratios = 0.25–1.0 and separations (a) = 0.288–5.481 au, except for Am stars, which were calculated for <0.3 au; see Section 4.3. The companion frequency for solar-type primaries is derived from the model of Raghavan et al. (2010), A-type primaries from the model of De Rosa et al. (2014) and this survey, A-type primaries using Am stars from Carquillat & Prieur (2007), and B-type primaries from the model of Rizzuto et al. (2013).
Paper: The Small Separation A-star Companion Population: First Results with CHARA/MIRC-X
Authors: Matthew De Furio, Tyler Gardner, John Monnier, Michael R. Meyer, Kaitlin Kratter, Gail Schaefer, Narsireddy Anugu, Claire L. Davies, Stefan Kraus, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Jacob Ennis
Figure caption: The detection limits derived from CANDID for each source are plotted in black, with the median value at each separation displayed in red. Detection limits correspond to the highest companion flux at a given separation over all position angles that results in a 5σ detection. Red circles represent the detections made in our survey at their given separation and contrast.
Paper: The Small Separation A-star Companion Population: First Results with CHARA/MIRC-X
Authors: Matthew De Furio, Tyler Gardner, John Monnier, Michael R. Meyer, Kaitlin Kratter, Gail Schaefer, Narsireddy Anugu, Claire L. Davies, Stefan Kraus, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Jacob Ennis
Figure caption: Derived detection limit for HD 31647 as a function of radius from the central star on both the MIRC-X and MYSTIC instruments. These data were collected simultaneously with 15 minute integrations.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Normalized line profiles of the Hα, Hβ, He I, Li I, [O I], and Na I lines. The lines with different colors indicate the different epochs (as listed in the upper right panel), the thick black line shows the average line profile, and the blue shaded area illustrates the variance profile in each panel.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Color–magnitude and color–color diagrams obtained from the SMARTS data. We drew the extinction corresponding to A  V  = 1 mag with black arrows. We indicated the values from the disk model of Figure 25 from Carpenter et al. (2001) with triangles. The open triangles represent a mass accretion rate of 10−8.5 M ⊙ yr−1, and the filled triangles indicate 10−7 M ⊙ yr−1. The three triangles correspond to inner disk hole sizes of 1, 2, and 4 R ⊙.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Light curves and periodogram of VW Cha in 2019. The top panel shows our near-infrared SMARTS JHK-band light curves. We show our optical I  C -band SMARTS photometry with red circles, the TESS light curve with black dots, and the nightly averaged ASAS-SN g-band data with green circles. The JHK- and g-band light curves are shifted along the y-axis with the values indicated in the figure. We marked the epochs of the spectroscopic observations with vertical orange (ESPRESSO) and purple (FEROS) lines. The bottom panel shows the Lomb–Scargle periodogram obtained from the TESS data.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Light curves and periodogram from 2021. In the top panel, the black dots show the TESS observations from 2021, and the green circles indicate the nightly averaged ASAS-SN g-band data. The bottom panel shows the Lomb–Scargle periodogram obtained from the 2021 TESS data.
Paper: Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Zsolt Regály, Viktória Fröhlich, József Vinkó
Figure caption: Mass loss as a function of time and orbital parameters by the end of the integration using the homologous expansion model (loss function and orbit in black). Colored lines show different linear mass-loss regimes. The secondary is a 1 M ⊕ planet. The gray line marks 60% of the ejecta mass, used for the constant mass-loss approximation.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Color–color diagram of VW Cha. Red circles are data from SMARTS observations at different epochs. The blue dashed line represents the CTTS locus. The orange solid and green dotted–dashed lines correspond to the zero-age main sequence and giant branch, respectively. The black arrow shows the vectorial shift from the CTTS locus for a source with 1 mag of extinction.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: The LSD profiles of VW Cha. The fitted Gaussians are indicated with orange curves. We indicated the individual Gaussian components with dashed curves when two components were fitted.
Paper: Accretion Variability of the Multiple T Tauri System VW Cha
Authors: Gabriella Zsidi, Eleonora Fiorellino, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, András Pál
Figure caption: Flux-calibrated and smoothed FEROS and ESPRESSO spectra.
Paper: Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3
Authors: Ying Qin, Yuan-Zhu Wang, Simone S. Bavera, Shichao Wu, Georges Meynet, Yi-Ying Wang, Rui-Chong Hu, Jin-Ping Zhu, Dong-Hong Wu, Xin-Wen Shu, Fang-Kun Peng, Han-Feng Song, Da-Ming Wei
Figure caption: Theoretical predictions of the marginal distributions (blue: CEE; magenta: CHE; green: SMT) of chirp mass (﹩{{ \mathcal M }}_{{\rm{c}}}﹩), mass ratio (q), and component spins (χ 1z  = χ 1, χ 2z  = χ 2, assuming both χ 1z  and χ 1z  are aligned to the direction of the orbital AM). The simulated data are obtained from the publicly released models in Zevin et al. (2021), except that for the CHE channel we extend the q distribution down to 0.5, which is in agreement with the studies in Mandel & de Mink (2016) and de Mink & Mandel (2016).
Paper: Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3
Authors: Ying Qin, Yuan-Zhu Wang, Simone S. Bavera, Shichao Wu, Georges Meynet, Yi-Ying Wang, Rui-Chong Hu, Jin-Ping Zhu, Dong-Hong Wu, Xin-Wen Shu, Fang-Kun Peng, Han-Feng Song, Da-Ming Wei
Figure caption: The posterior distributions for GW190517_055101 inferred by LVK’s default prior (gray) and the CHE prior (magenta). The inner and outer solid circles in the 2D plots mark the 68% and 90% credible regions, respectively.
Paper: Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3
Authors: Ying Qin, Yuan-Zhu Wang, Simone S. Bavera, Shichao Wu, Georges Meynet, Yi-Ying Wang, Rui-Chong Hu, Jin-Ping Zhu, Dong-Hong Wu, Xin-Wen Shu, Fang-Kun Peng, Han-Feng Song, Da-Ming Wei
Figure caption: Violin plot showing marginal posterior distributions of individual spins (upper panel) and mass ratios (lower panel) inferred with LVK’s default prior and the CHE prior. These selected events have odd ratios larger than 1/3 for the CHE channel. For brevity, we omit the suffix of the event name.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Fractional populations of metastable states of C-like Fe evaluated as a function of the relative abundance of N-like Fe at conditions close to those of our experiment (E = 2000 eV, ﹩\mathrm{log}{n}_{e}=10.5﹩). The metastable level populations weakly increase together with the relative fraction of N-like Fe. There is no dependence on the B-like Fe abundance (not shown).
Paper: Searching for Candidates of Coalescing Binary Black Holes Formed through Chemically Homogeneous Evolution in GWTC-3
Authors: Ying Qin, Yuan-Zhu Wang, Simone S. Bavera, Shichao Wu, Georges Meynet, Yi-Ying Wang, Rui-Chong Hu, Jin-Ping Zhu, Dong-Hong Wu, Xin-Wen Shu, Fang-Kun Peng, Han-Feng Song, Da-Ming Wei
Figure caption: The same as Figure 3, but for the results inferred with the SMT prior. The selected events have odd ratios larger than three for the SMT channel.
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Fractional populations of metastable states of C-like Fe evaluated as a function of the electron density at an electron energy close to that of our experiment (E = 2000 eV). The N-like and C-like fractions are set to be equal.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Histograms of the S/N in the post-merger phase of BBH binaries (left panel) and NSBH binaries (right panel), for 1 yr of data. For BBHs the computation is performed using the IMRPhenomHM waveform, while for NSBH systems we adopted IMRPhenomNSBH.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Histograms of the parameter errors for BNSs with the ET+2CE network configuration, using the waveform model IMRPhenomD_NRTidalv2, and sampling the tidal deformability uniformly in the interval [0, 2000] (red line), or assuming for all BNSs a common equation of state, chosen to be APR4 (violet) or ALF2 (orange).
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Histograms of the parameter errors for NSBHs with the ET+2CE network configuration, using the waveform model IMRPhenomNSBH, and sampling the BH mass and system redshift from our baseline distribution, and from two distributions taken from Broekgaarden et al. (2021). The tails of the distributions featuring extremely large values of the relative errors, as in some of the panels, simply represent the contribution of events for which the Fisher matrix approximation cannot be trusted.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Scatter plots of the observed NSBH population at 3G detectors. On the top row, we report the results for ET alone; and in the bottom, for the ET+2CE network. In each row, the left panel shows the distribution of errors on the luminosity distance and sky location as a function of redshift, the central panel the distribution of errors on the luminosity distance, and detector-frame chirp mass as a function of redshift; and the right panel, the distribution of errors on the source-frame chirp mass and symmetric mass ratio as a function of the total source-frame mass. The numbers reported on the dashed lines refer to the fraction of observed events lying inside the corresponding region.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Histograms of the parameter errors for BNSs with the ET+2CE network configuration, using the full inspiral-merger-ringdown waveform model IMRPhenomD_NRTidalv2 and the 3.5 restricted PN model TaylorF2 with tidal effects.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Histograms of the parameter errors for NSBH with the ET+2CE network configuration, using the full inspiral-merger-ringdown waveform model IMRPhenomNSBH and the 3.5 restricted PN model TaylorF2 with tidal effects.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Comparison of cumulative distributions of the errors on the detector-frame chirp mass, symmetric mass ratio, luminosity distance, 90% sky localization, and spin components along the z -axis, for BNS observed at ET, with different choices to quantify the uncertainty. The default choice for this paper, ϵ < 0.05, corresponds to the orange curve.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 25, for a network of ET and two CE.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We show the radial structure of the disk scale aspect ratio (h/r), gas temperature T gas, plasma-β (=p gas/p mag), radial velocity ∣v  r ∣, angular velocity Ω, and specific angular momentum u  φ . All quantities are disk-averaged. The MAD model has a thinner (i.e., lower h/r), more magnetized (smaller β), hotter (higher T gas), and more sub-Keplerian (lower Ω and smaller u  ϕ ) inner disk compared to the SANE model. The time averages are obtained over the final 5 × 104 r g/c of time for each simulation.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We show the streamlines of the total angular momentum flux ﹩{\dot{J}}_{\mathrm{tot}}﹩, the (mostly inward) advective flux ﹩{\dot{J}}_{\mathrm{adv}}﹩, and the (outward) stress-induced flux ﹩{\dot{J}}_{\mathrm{stress}}={\dot{J}}_{\mathrm{tot}}-{\dot{J}}_{\mathrm{adv}}﹩, for the MAD (top) and SANE (bottom) simulations, with gas density in color. All quantities are t- and φ-averaged and θ-symmetrized in order to reduce the effects of turbulent eddies. Larger-scale eddies persist in the SANE model as seen from the ﹩{\dot{J}}_{\mathrm{tot}}﹩ streamlines at r > 60r g. The disk scale height is indicated with red dashed lines (see Figure 8), which demarcate the disk region, outside of which disk winds can transport angular momentum outward if strong enough. On average, the outward stress-induced angular momentum transport in the MAD model is more vertically oriented while in the SANE model, the outward flux is generally more equatorial in nature (compare the panels in the rightmost column, and also see Figure 11).
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: Weakly magnetized disks (SANE, orange) and magnetically arrested disks (MAD, blue) evolve quite differently over time. We show the time evolution of fluxes in the SANE and MAD simulations: the accretion rate ﹩\dot{M}﹩, the dimensionless magnetic flux ϕ, the specific radial flux of the angular momentum ﹩{\dot{J}}_{\mathrm{int}}^{r}/\dot{M}﹩, the outflow power efficiency ﹩{P}_{\mathrm{out}}/\dot{M}{c}^{2}﹩, and the disk barycentric radius r disk. We calculate ﹩\dot{M}﹩, ﹩{\dot{J}}_{\mathrm{tot}}﹩, and P out at 5r g in order to avoid any spurious effects from density floors. The magnetic flux is estimated at the event horizon.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We compare the normalized net inflow mass accretion rate ﹩\dot{M}﹩ and the mass outflow rate ﹩{\dot{M}}_{\mathrm{out}}﹩ for the MAD (thick lines) and SANE (thin lines) models, time-averaged over the final 5 × 104 r g/c of time. Inward (outward) fluxes are indicated by solid (dashed) lines. We perform two types of calculations for the mass outflow rate: ﹩{\dot{M}}_{\mathrm{out},\mathrm{avg}}﹩, where we apply constraints on the t- and φ-averaged outward radial velocity (v  r  > 0) and specific radial energy flux (μ e > 0), and ﹩{\dot{M}}_{\mathrm{out},\mathrm{inst}}﹩, where the constraints are applied on the instantaneous values of v  r  and μ e at each time. These two calculations provide lower and upper bounds on the true ﹩{\dot{M}}_{\mathrm{out}}﹩. Both models achieve an average outflow rate between 60% and 80% of the net mass inflow rate at r ≈ 100r g, showing that winds do not efficiently remove gas from the disk.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: There is significant evolution of the radial disk structure over time in both models. We show the time-averaged disk gas density ρ, surface density Σ, and mass accretion rate ﹩\dot{M}﹩, calculated for four time chunks (identified by color). By the final time chunk, each model achieves inflow–outflow equilibrium out to at least 100–150r g, as seen from the ﹩\dot{M}﹩ profiles. Radial power-law fits to ρ and Σ are shown over a radius range where the disk scale aspect ratio is roughly constant in the two models (see Figure 8).
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We show the angle between the poloidal vector ﹩{\dot{J}}_{\mathrm{stress}}^{i}﹩ and the radial vector  r  at three different radii: 20r g, 40r g, and 60r g. For the MAD model, the angular separation is negative, with ﹩{\dot{J}}_{\mathrm{stress}}﹩ reaching a maximum offset of ∼20° counterclockwise (clockwise) from  r  in the upper (lower) hemisphere of the wind region. The sign of the deviation indicates the vertical outward transport of angular momentum. We see the opposite behavior in the SANE model, which is consistent with the horizontal transport of angular momentum. The vertical dashed lines indicate the disk scale aspect ratio for both models at each radius.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: The MAD is, on average, magnetic pressure dominated within the inner few gravitational radii while the SANE disk is always thermal pressure supported. We show the radial profiles of the time- and disk-averaged thermal and magnetic pressure as well as the different components of the magnetic pressure. The radial component of the magnetic pressure of the MAD model exceeds the toroidal component, indicating that the inner disk contains strong poloidal fields. The time averaging is done over the same period in Figure 8.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We show the gas density and velocity streamlines for the SANE (left side) and MAD (right side) accretion flows, time-averaged and azimuthally averaged over the final 50,000r g/c for each simulation. We also symmetrize the data in the θ-direction across the disk midplane. We indicate the magnitude of the velocities using the line widths of the streamlines: light (bold) lines indicate low (high) velocities. Outgoing streamlines in the MAD model indicate a prominent wind component.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We see gas infall in the polar regions of the SANE simulation at late times. We show the gas density ρ at 2 × 105 r g/c with black lines indicating the velocity streamlines. The disk also undergoes a change in orientation at times as large-scale eddies accrete at random times during the simulation.